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Le Champ Du Cygne ...Ou La Spectroscopie Par L'exemple !

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Le Champ Du Cygne ...Ou La Spectroscopie Par L'exemple ! Le champ du Cygne ...ou la Spectroscopie par l'exemple ! Olivier THIZY WETAL, Vaulx-en-Velin 10 novembre 2013 Photo: Jim Edlin, OHP la constellation du Cygne ● Zeus en pris la forme pour séduire Léda... Pollux & Hélène sont leurs enfants ! ● la "croix du Nord", bien visible la nuit en été et le soir en automne ● DEC +27° --> +60° è ● 16 constellation en taille ● une superbe étoile double: Albiréo Photo fond: Jim Edlin (OHP) Source: Johannes Hevelius (1611-1687) Uranographia [1690, publié post mortem par son épouse] Albiréo, une double colorée beta Cygni (Albireo) Pourquoi ces couleurs ? Photos: Jim Edlin (Cygne), Hunter Wilson (Albireo) Faisons appel à un "ami"... Décomposition de la lumière ● Isaac Newton : un pionnier ● 1670: expérience du prisme ● “fente” cercle de 6mm: λ/∆λ ~10 ! ● Observation d'un „spectre“ Arc-en-ciel naturel Photo: F. Cochard Arc-en-ciel artificiel Photos: C. Buil / O. Thizy Spectre électromagnétique ● 1800: W. Hershel découvre l'Infra-Rouge ● 1801: J. W. Ritter découvre l'Ultra-Violet ● 1801: T. Young, nature ondulatoire de la lumière Source: Benjamin ABEL & images libres Les premiers spectres: le Soleil ● William Wollaston (1766-1828) ● ~150 ans après Newton ! ● Premières observations (en 1802) de raies sombres ● A démontré l'importance de la largeur de fente ● Joseph Fraunhofer (1787-1826) ● Fabriquant de verre de grand qualité ● A, B (Ha), C, D (doublet du sodium)... H, K (Calcium) ● Catalogue de ~600 raies en 1814 ● Observa aussi des planètes et quelques toiles ● Edmon Becquerel (1820-1891) ● Première photographie du spectre solaire (13 juin 1842) le spectre du Soleil en visuel (c) Robin Leadbeater le sodium dans tous ses états Sel Allumette Cornichon ! Lampe de rue Soleil Sirius Crédits: C. Buil / B. Minster Analyses spectroscopiques... Spectres: C. Buil; photo: O. Thizy (stage OHP) à consommer avec modération ! Analyses spectroscopiques... Spectres: C. Buil; photo: O. Thizy (stage OHP)... et A. Franquin ! à consommer avec beaucoup de modération ! Analyse chimique & Spectroscopie ● Léon Foucault (1819-1868) ● Comparaison entre spectre sur Terre et spectre du Soleil (raies du sodium, 1849) ● Gustav Kirchhoff ● En parallèle, il expérimenta avec le sel et publia en 1859 que le sodium devait exister dans l'atmosphère du Soleil! ● Un résultat théorique clef: les lois de Kirchhoff ● Robert Bunsen (1811-1899) ● Université de Heidelberg (comme Kirchhoff) ● Ensemble ils publièrent en 1860 un papier sur «l'analyse chimique par observation spectroscopique»; et en 1861-1863 l'analyse de plusieurs éléments chimiques et un travail sur le spectre solaire la Spectroscopie est née Photos : Wikipedia / O. Thizy Travaux Pratiques... Le spectrographe Alpy 600 Albiréo (1) (1) Profils de formes différentes ? (2) Raies en absorptions ? (3) Raie en émission (bet Cyg B) ? (3) (1) (2) Elémentaire mon cher Watson... merci Mr Kirchhoff ! Loi de Kirchhoff #1 1 2 3 Un gaz à pression élevé, un liquide ou un solide, s'ils sont 1 chauffés, émettent un rayonnement continu qui contient toutes les couleurs; Un gaz à basse pression et basse température, s'il est situé entre 2 une source de rayonnement continu et un observateur, absorbe certaines couleurs (spectre de raies en absorption). Un gaz chaud à basse pression émet un rayonnement uniquement 3 pour certaines couleurs (spectre de raies en émission) Profil de Planck ➢La loi de Stefan: Intensité (sous la courbe) = Constante * T4 ➢La loi de Wien: λ max * Température = Constante (2900 µm.K) ==>Température = Couleur !!! Domaine Visible = 400-700nm (4000A-7000A) profil vs. température effective Profil de Plank 12.000 K 10.000 K é 8.000 K t i s n e t 5.000 K n I 1000 2000 3000 4000 5000 6000 7000 8000 9000 10000 Longueur d'onde (angstroms) TP: VisuelSpec "autoPlanck" 4000K Wikipedia: 4080K 13000K Wikipedia: 13200K Attention: vue très partielle du spectre Source: Getting the measure of the stars (WA Cooper & EN Walker) Loi de Kirchhoff #2 1 2 3 Un gaz à pression élevé, un liquide ou un solide, s'ils sont 1 chauffés, émettent un rayonnement continu qui contient toutes les couleurs; Un gaz à basse pression et basse température, s'il est situé entre 2 une source de rayonnement continu et un observateur, absorbe certaines couleurs (spectre de raies en absorption). Un gaz chaud à basse pression émet un rayonnement uniquement 3 pour certaines couleurs (spectre de raies en émission) Atmosphère stellaires raies d'hydrogène (visualSpec) H / K (Calcium) Hδ Hβ Triplet du Magnésium Profil spectral : O. janvier Thizy, 2007 ; Lhires –III 300tt/mm; RebelDigital / EOS300D Spectre solaire Doublet du Sodium Hα Classification spectrale ● Quelques précurseurs: Lewis Rutherfurd (1816-1892), Angelo Secchi (1818-1878), William Huggins (1824-1910), Hermann Carl Vogel (1841-1907) ● Un travail essentiel: le catalogue Henry Drapper (HD) à Harvard ● Edward Pickering (1846-1919) et son “harem”; fondateur de l'AAVSO ● Williama Fleming (1857-1911): types A...Q; 26000 spectres ● Antonia Maury (1866-1952): types I...XX; première à mettre le type O devant le type A ● Annie Cannon (1863-1941): types: OBAFGKM – Sous-division décimale (B0..9) – ~400000 spectres catalogués !!! ● 1943: “Atlas of Stellar Spectra” par William Morgan, Philip Keenan, & Edith Kellman [MKK] ● Type spectral du catalogue HD: OBAFGKM ● Notion de Classe de Luminosité I...V A.J. Cannon Le Top 5 du Cygne A2Iae K0III F8Iab K3II B8Ve B9.5IV Classification spectrale dans le Cygne hydrogène 68 Cyg O5V lam Cyg B5V 40 Cyg A3V the Cyg F4V zet Cyg G8II 61 Cyg K5V 19 Cyg M2IIIa H/K Na (D) atmosphère Oh, Be A Fine Girl/Guy... Kiss Me ! "Visibilité" des raies vs. Température Température de plus en plus froide Classe de luminosité Alp Cyg (A2I) 40 Cyg (A3V) Diagramme HR ● Ejnar Hertzsprung (1873-1967) & Henry Russell (1877-1957) ● Diagramme Couleur/Luminosité (première publication en 1911) Dessin : CLEA Loi de Kirchhoff #3 1 2 3 Un gaz à pression élevé, un liquide ou un solide, s'ils sont 1 chauffés, émettent un rayonnement continu qui contient toutes les couleurs; Un gaz à basse pression et basse température, s'il est situé entre 2 une source de rayonnement continu et un observateur, absorbe certaines couleurs (spectre de raies en absorption). Un gaz chaud à basse pression émet un rayonnement uniquement 3 pour certaines couleurs (spectre de raies en émission) Spectroscope pédagogique Albiréo b: une étoile Be ● Etoile de type B, non super-géante, montrant ou ayant montré une raie de Balmer en émission ● Découvertes en 1866 par le père Sechi: gamma Cas, beta Lyrae... ● Disque de matière expulsée de l'étoile, rémettant de l'énergie qu'il a absorbé du rayonnement UV de cette étoile ● Cf présentation de Valérie Desnoux du samedi 9 nov... Cf: http://www.shelyak.com/dossier.php?id_dossier=24 Nébuleuse Planétaire: NGC7027 NGC 7027 Nébuleuse Planétaire: NGC7027 NGC7027: identification des raies © O. Thizy Cf la 'bible': http://www.astronomie-amateur.fr/feuilles/Spectroscopie/NGC2392.html Hγ [O III] He II Hβ [O III] [O III] He II [N II] He I [O I] [N II] Hα [N II] [S II] [Ar III] Np: calcul de température & densité Te = 10933 ±174 K Hα 6563 Ne = 2537 ±61 e-/cm3 [OIII] 5007 [NII] 6583 Hβ [NII] 4861[OIII] 6548 4959 HeI HeI 5876 6678 Spectre de M42 - Lhires III (150tt/mm) + KAF1600 / Acquisition: Benjamin Mauclaire / Traitement: Olivier Thizy Cf: http://bmauclaire.free.fr/astronomie/spectro/atlas/nd/m42/ étoiles de Wolf Rayet WC7p+O5 WR 140 WR 136 WN6h évolution des Wolf Rayet © James Lequeux: naissance, vie et mort des étoiles (EDP Sciences) P Cygni P Cygni Hα 1 mag ! Hγ Hβ He I Nova Del 2013 ● Détectée le 14 août 2013 ● Pas à proprement parlé dans le Cygne, mais très proche... :-) ● Cf présentations de Steve Shore & François Teyssier du 9-nov ● Noter le profil "P Cygni" au début du phénomène Nova Del 2013 Profil „P Cygni“ Effet Doppler - Fizeau Expansion des galaxies (Δ λ) = = ν Décalage vers le rouge λ (red shift) c Application de l'effet Doppler: profil P Cygni v A A: émission du gaz v étoile B v v ~ c (λ -λ )/λ Enveloppe A B: absorption A B B en expansion par le gaz λ λ v B A R Cyg: type S, proche du maximum ● Type spectral S: géante rouge en fin de vie; à mi chemin entre type M & étoile "carbonée" ● Variable de type Mira R Cyg ZrO (monoxyde de zirconium) Hβ Hα Na V460 Cyg: type C6,3 V460 Cyg C2 ● Type spectral C6,3 : étoile carbonée ● Teff ~3200K ● intensité moyenne des bandes de C2 Etoile symbiotique: CH Cyg Hα Hδ Hγ Hβ ● Géante rouge + naine blanche ● Transfert de masse CH Cyg Autre étoile symbiotique: BF Cyg Hα Hδ Hγ Hβ BF Cyg En résumé La lumière des étoiles nous renseigne sur : • leur température [profile global] • leur composition et les conditions physiques d'excitation ou d'ionisation (ie temperature) [raies visibles] • leur composition chimique quantitative (abondance), la pression, la gravité [intensité et forme des raies] Mais aussi sur : • les mouvements [effet Doppler] ● vitesse radiale ● rotation ● expansion Schéma : Bengt Gustafsson Conclusions ● La spectroscopie est un «jeu scientifique» ● C'est un domaine en plein essort ● le matériel est disponible sur étagère ● les logiciels se développent et se simplifient ● des tutoriaux et des projets décrits sur le web ● la littérature va suivre ● une entre-aide active ● Devenez détective d'un soir... ● ...et entrez dans le monde des Pro/Am ! ARAS group http://www.astrosurf.com/aras/ ARAS forum http://www.spectro-aras.com/forum/ Spectro-L discussion http://groups.yahoo.com/group/spectro-l/ Shelyak Instruments http://www.shelyak.com/ .
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